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When solids, liquids, or condensed gases are heated sufficiently, they radiate some of the excess energy as light. Photons produced in this manner have a range of energies, and thereby produce a continuous spectrum in which an unbroken series of wavelengths is present.
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Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
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Ultraviolet–visible (UV–visible or UV–Vis) spectroscopy is an analytical technique that investigates the interaction between matter and UV–Vis light within the electromagnetic spectrum. This method is widely used for its versatility, simplicity, and relatively quick data acquisition, making it valuable for both qualitative and quantitative analysis. When UV–Vis radiation passes through a material,  molecules absorb light depending on the energy required for...
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Atomic emission spectroscopy (AES) is an analytical technique used to determine the elemental composition of a sample by analyzing the light emitted from excited atoms. In AES, atoms in a sample are excited to higher energy levels by thermal energy from high-temperature sources, such as plasma, arcs, or sparks. When these excited atoms return to lower energy states, they emit light at specific wavelengths characteristic of each element. The resulting atomic emission spectrum, which consists of...
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No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
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Electromagnetic (EM) radiation can be considered an oscillating electric and magnetic field propagating through a medium that can interact with matter in its path. The electric field in the radiation can interact with electrical charges in the atoms or molecules in the matter. On the other hand, the magnetic field can interact with the magnetic field in the atomic nucleus. The study of the interaction between electromagnetic radiation and matter is termed spectroscopy. Spectroscopy is the study...
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Updated: Sep 4, 2025

Characterizing Far-infrared Laser Emissions and the Measurement of Their Frequencies
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Emisión extendida de ultravioleta lejana en galaxias enanas distantes

Anshuman Borgohain1, Kanak Saha2, Bruce Elmegreen3

  • 1Department of Physics, Tezpur University, Napaam, India. ayush.borgohain@gmail.com.

Nature
|July 21, 2022
PubMed
Resumen

Observamos la formación de estrellas extendidas en galaxias enanas azules compactas usando el telescopio AstroSat. Esto sugiere una acumulación de gas y una inestabilidad gravitacional en sus regiones exteriores.

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Área de la Ciencia:

  • Astronomía y astrofísica
  • Formación y evolución de las galaxias

Sus antecedentes:

  • Las galaxias enanas compactas azules (BCD) son de baja luminosidad, pobres en metales y centralmente concentradas, con grupos de formación estelar.
  • La observación de la formación de BCD es un desafío debido a la atenuación y el pequeño tamaño a altos desplazamientos al rojo.
  • Las observaciones intermedias de desplazamiento al rojo son cruciales para estudiar las primeras etapas evolutivas de los BCD, especialmente las regiones externas influenciadas por la acreción de gas.

Objetivo del estudio:

  • Para investigar los procesos de formación de las galaxias enanas azules compactas.
  • Analizar la actividad de formación estelar en las regiones externas de los BCD en desplazamientos al rojo intermedios.

Principales métodos:

  • Observaciones de 11 BCD en el campo GOODS Sur utilizando el Telescopio de Imágenes Ultravioleta en AstroSat.
  • Análisis de la emisión ultravioleta lejana (FUV) y comparación con los datos ópticos del Telescopio Espacial Hubble.
  • Corrección de la función de dispersión de los puntos de los instrumentos para determinar los perfiles radiales intrínsecos de la emisión de UVF.

Principales resultados:

  • Se ha detectado un exceso de emisión ultravioleta lejana (UVL) en las regiones exteriores de 11 BCD con desplazamientos al rojo de 0,1 a 0,24.
  • Los perfiles radiales de emisión intrínseca de FUV muestran longitudes de escala más grandes que las contrapartes ópticas para diez BCD.
  • La estructura FUV agrupada indica inestabilidad gravitatoria en los discos externos.

Conclusiones:

  • La formación de estrellas extendida en discos de acreción cósmica se sugiere por perfiles FUV poco profundos.
  • La inestabilidad gravitacional en los discos FUV externos impulsa la migración hacia el interior de los grupos a través de la fricción dinámica.
  • Las regiones externas del BCD están evolucionando activamente, impulsadas por la acreción de gas y la dinámica interna.